Worlds in Eruption
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Investigating Mineral Stability Under Venus Conditions: a Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville
University of Arkansas, Fayetteville ScholarWorks@UARK Theses and Dissertations 5-2016 Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville Follow this and additional works at: http://scholarworks.uark.edu/etd Part of the Geochemistry Commons, Mineral Physics Commons, and the The unS and the Solar System Commons Recommended Citation Kohler, Erika, "Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies" (2016). Theses and Dissertations. 1473. http://scholarworks.uark.edu/etd/1473 This Dissertation is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Space and Planetary Sciences by Erika Kohler University of Oklahoma Bachelors of Science in Meteorology, 2010 May 2016 University of Arkansas This dissertation is approved for recommendation to the Graduate Council. ____________________________ Dr. Claud H. Sandberg Lacy Dissertation Director Committee Co-Chair ____________________________ ___________________________ Dr. Vincent Chevrier Dr. Larry Roe Committee Co-chair Committee Member ____________________________ ___________________________ Dr. John Dixon Dr. Richard Ulrich Committee Member Committee Member Abstract Radar studies of the surface of Venus have identified regions with high radar reflectivity concentrated in the Venusian highlands: between 2.5 and 4.75 km above a planetary radius of 6051 km, though it varies with latitude. -
Styles of Deformation in Ishtar Terra and Their Implications
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 97, NO. El0, PAGES 16,085-16,120, OCTOBER 25, 1992 Stylesof Deformationin IshtarTerra and Their Implications Wn.T.TAMM. KAU•A,• DOAN•L. BINDSCHAD•-R,l ROBERT E. GPaM•,2'3 VICKIL. HANSEN,2KARl M. ROBERTS,4AND SUZANNE E. SMREr,AR s IshtarTerra, the highest region on Venus, appears to havecharacteristics of both plume uplifts and convergent belts.Magellan imagery over longitudes 330ø-30øE indicates a great variety of tectonicand volcanic activity, with largevariations within distances of onlya few 100km. Themost prominent terrain types are the volcanic plains of Lakshmiand the mountain belts of Maxwell,Freyja, and Danu. Thebelts appear to havemarked variations in age. Thereare also extensive regions of tesserain boththe upland and outboard plateaus, some rather featureless smoothscarps, flanking basins of complexextensional tectonics, and regions of gravitationalor impactmodifica- tion.Parts of Ishtarare the locations of contemporaryvigorous tectonics and past extensive volcanism. Ishtar appearsto be the consequence of a history of several100 m.y., in whichthere have been marked changes in kinematic patternsand in whichactivity at any stage has been strongly influenced by the past. Ishtar demonstrates three general propertiesof Venus:(1) erosionaldegradation is absent,leading to preservationof patternsresulting from past activity;(2) manysurface features are the responses ofa competentlayer less than 10 km thick to flowsof 100km orbroaderscale; and (3) thesebroader scale flows are controlled mainly by heterogeneities inthe mantle. Ishtar Terra doesnot appear to bethe result of a compressionconveyed by anEarthlike lithosphere. But there is stilldoubt as to whetherIshtar is predominantlythe consequence of a mantleupflow or downflow.Upflow is favoredby the extensivevolcanic plain of Lakshmiand the high geoid: topography ratio; downflow is favoredby the intense deformationof themountain belts and the absence of majorrifts. -
User Guide to the Magellan Synthetic Aperture Radar Images
https://ntrs.nasa.gov/search.jsp?R=19950018567 2020-06-16T07:22:10+00:00Z User Guide to the Magellan Synthetic Aperture Radar Images Stephen D. Wall Shannon L. McConnell Craig E. Left Richard S. Austin Kathi K. Beratan Mark J. Rokey National Aeronautics and Jet Propulsion Laboratory Space Administration California Institute of Technology Scientific and Technical Pasadena, California Information Branch NASA Reference Publication 1356 March 1995 This publication was prepared at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Contents Iri Introduction .................................................................................................................................................................... 1 I_1 The Spacecraft ................................................................................................................................................................ 2 IB Mission Design ................................................................................................................................................................ 4 D Experiment Description ................................................................................................................................................ 15 B Mission Operations ....................................................................................................................................................... 17 [] Notable Events and Problems ..................................................................................................................................... -
Saturn's Little Ice Moon Enceladus Looks Very Alien to Ter- Restrial
22 23 The UN has declared 2009 the International Year of Astronomy to celebrate the 400th Enceladus is the dark spot inside the bright flare at the centre of Saturn's E ring. Plumes anniversary of Galileo Galilei’s first astronomical observations with a telescope and of ice and water vapour are erupting off the moon to form this ring. the publication of Astronomia Nova by Johannes Kepler. In that connection, NPD pal- (Photo: Nasa/JPL/Space Science Institute) aeontologist Robert W Williams looks at a Saturn moon’s geology. Hot and cold Saturn’s little ice moon Enceladus looks very alien to ter- restrial geologists. Like Earth, however, this world is crunchy on the outside and soft on the inside. A warm inte- rior requires energy, and an unearthly source is pumping up its heat. 24 25 Enceladus is a tectonically active moon of Saturn and consists mainly of water ice. The prominent tectonic divide visible near the top of the image is Labtayt Sulci, a one- kilometre-deep rift. Note the absence of craters over large areas. (Photo: Nasa/JPL/Space Science Institute) Saturn photographed from within its shadow. Details of the ring system become more distinct when the Sun’s illumination is from the back. Encircling the entire system is the E ring. The icy plumes of Enceladus, whose eruptions supply the ice dust of the E ring, betray the moon's position on the ring's left-hand edge. Located 1.3 billion kilometres away, just above the leftmost edge of the brighter main rings, is the pale blue dot of Earth. -
Volcanism and Tectonism in Rusalka Planitia and Atla Regio, Venus; M
LPSC xn/ 767 VOLCANISM AND TECTONISM IN RUSALKA PLANITIA AND ATLA REGIO, VENUS; M. G. Lancaster and J. E. Guest (University of London Observatory, University College London, London, NW7 2QS, U. K.). In order to investigate the relationships between volcanism and tectonism in Rusalka Planitia and Atla Regio, the geology of four adjacent Cycle 1 Magellan ClMIDRs has been mapped (C100N180, C115N180, C115N197, and C100N197). These cover nearly 12 x 106 km2 between latitudes 7.6 S and 22.6 N, and longitudes 171.4 to 206.2 E. This region was chosen because it contains nearly all the types of volcanic and tectonic features observed on Venus, and covers plains as well as highlands. The western half of the region comprises most of the volcanic plains of Rusalka Planitia, which are characterized by a large-scale pervasive fabric of NW-SE trending sinuous ridges that resemble lunar and martian wrinkle ridges [I]. A NW-SE to N-S trending deformation belt occupies the SW comer of C100N180, and contains several coronae including Eigin Corona (5.0 S, 175.0 E). The belt is the source for large, radar-bright, plains forming, flood lava flow fields. A similar collection of corona-like centers and deformation belts composed largely of ridges, is found in the NE comer of C115N197, where an extensive collection of lava flow fields is also present. Other smaller regions of radar-bright lava lie scattered across the plains. A number of N-S to NNW-SSE trending ridge belts occupy the north-central part of these plains. -
Tidal Forces in the Solar System - Course: HET 602, April 2002 Instructor: Dr
Essay: Tidal forces in the Solar System - Course: HET 602, April 2002 Instructor: Dr. Sarah Maddison - Student: Eduardo Manuel Alvarez Tidal forces in the Solar System Introduction As anywhere else in the Universe, gravity is the basic and fundamental principle that rules the shape and permanent motion of all the celestial bodies inside the Solar System. No matter the type of planet, moon, asteroid or comet, gravity accounts for the main parameters of each orbit, which can be calculated by considering each body as a point mass. But there are other gravitational effects, those coming from the fact that actual bodies do have internal dimensions, which become the major cause for specific and unique characteristics of a lot of members of the Solar System. Such effects are derived from differential gravitational forces or "tidal forces", which not only have dramatically affected the development of the present state of the Solar System, but will endlessly continue reshaping it as well. Tidal forces fundamentals According to Newton's law of universal gravitation, the attractive force (F) reciprocally exerted between two masses (m, M) being separated at a distance (d) is: GMm F = d 2 where G is the universal constant of gravitation. Inside a celestial body, the gravitational force exerted by the distant mass (M) on any small element of mass (m) varies as its relative position changes, having an overall distribution as illustrated in Figure 1. Figure 1 FigureFigure 2 2 Forces relative to the distant mass ForcesForces relative relative to deto thecenter center Page 1 of 6 Essay: Tidal forces in the Solar System - Course: HET 602, April 2002 Instructor: Dr. -
Venus Lithograph
National Aeronautics and and Space Space Administration Administration 0 300,000,000 900,000,000 1,500,000,000 2,100,000,000 2,700,000,000 3,300,000,000 3,900,000,000 4,500,000,000 5,100,000,000 5,700,000,000 kilometers Venus www.nasa.gov Venus and Earth are similar in size, mass, density, composi- and at the surface are estimated to be just a few kilometers per SIGNIFICANT DATES tion, and gravity. There, however, the similarities end. Venus hour. How this atmospheric “super-rotation” forms and is main- 650 CE — Mayan astronomers make detailed observations of is covered by a thick, rapidly spinning atmosphere, creating a tained continues to be a topic of scientific investigation. Venus, leading to a highly accurate calendar. scorched world with temperatures hot enough to melt lead and Atmospheric lightning bursts, long suspected by scientists, were 1761–1769 — Two European expeditions to watch Venus cross surface pressure 90 times that of Earth (similar to the bottom confirmed in 2007 by the European Venus Express orbiter. On in front of the Sun lead to the first good estimate of the Sun’s of a swimming pool 1-1/2 miles deep). Because of its proximity Earth, Jupiter, and Saturn, lightning is associated with water distance from Earth. to Earth and the way its clouds reflect sunlight, Venus appears clouds, but on Venus, it is associated with sulfuric acid clouds. 1962 — NASA’s Mariner 2 reaches Venus and reveals the plan- to be the brightest planet in the sky. We cannot normally see et’s extreme surface temperatures. -
Venera-D Landing Sites Selection and Cloud Layer Habitability Workshop Report
1 Venera-D Landing Sites Selection and Cloud Layer Habitability Workshop Report IKI Moscow, Russia October 2-5, 2019 Space Science Research Institute (IKI), Russian Academy of Science, Roscosmos, and NASA http://venera-d.cosmos.ru/index.php?id=workshop2019&L=2 https://www.hou.usra.edu/meetings/venera-d2019/ 2 Table of Contents Introduction ...................................................................................................................................................... 6 Final Agenda .................................................................................................................................................. 10 Astrobiology Special Collection of papers from the workshop .................................................... 14 Technical Report: Venera-D Landing Site and Cloud Habitability Workshop ......................... 15 1.0 Missions to Venus .......................................................................................................................... 15 1.1 Past and Present ................................................................................................................................. 15 1.1.1 Available Instruments and Lessons Learned Surface Geology ........................................................... 15 1.1.2 Available Instruments and Lessons Learned for Cloud Habitability ............................................... 16 1.2 Future Missions .................................................................................................................................. -
6Th Grade Science: Orbital Periods
Science Virtual Learning 6th Grade Science: Orbital Periods May 1, 2020 6th Grade Science Lesson: May 1,2020 Objectives/Learning Targets: ● Students will display orbital periods of the solar system’s objects. Essential Question: ● What is the appropriate way to display orbital periods of objects in our solar system? Warm Up ● First,record your answers to the questions below on a piece of paper. 1. What is an orbit? 2. What causes an orbit to happen? 3. How long does it take the Earth to orbit (revolve) the Sun? 4. What is the difference between a rotation and revolution? ● Next, watch this video: The Rotation and Revolution of Earth and compare your answers to the information you learn from the video. Warm Up Answer Key 1. What is an orbit? Answer: An orbit is a regular, repeating path that an object in space takes around another one. 2. What causes an orbit to happen? Answer: Orbits are the result of a perfect balance between the forward motion of a body in space, such as a planet or moon, and the pull of gravity on it from another body in space, such as a large planet or star. An object with a lot of mass goes forward and wants to keep going forward; however, the gravity of another body in space pulls it in. There is a continuous tug-of-war between the one object wanting to go forward and away and the other wanting to pull it in. 3. How long does it take the Earth to orbit the Sun? Answer: Earth orbits the Sun at an average distance of 149.60 million km (92.96 million mi), and one complete orbit takes 365.256 days. -
Surface Processes in the Venus Highlands: Results from Analysis of Magellan and a Recibo Data
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 104, NO. E], PAGES 1897-1916, JANUARY 25, 1999 Surface processes in the Venus highlands: Results from analysis of Magellan and A recibo data Bruce A. Campbell Center for Earth and Planetary Studies, Smithsonian Institution, Washington, D.C. Donald B. Campbell National Astronomy and Ionosphere Ceiitei-, Cornell University, Ithaca, New York Christopher H. DeVries Department of Physics and Astronomy, University of Massachusetts, Amherst Abstract. The highlands of Venus are characterized by an altitude-dependent change in radar backscattcr and microwave emissivity, likely produced by surface-atmosphere weathering re- actions. We analyzed Magellan and Arecibo data for these regions to study the roughness of the surface, lower radar-backscatter areas at the highest elevations, and possible causes for areas of anomalous behavior in Maxwell Montes. Arecibo data show that circular and linear radar polarization ratios rise with decreasing emissivity and increasing Fresnel reflectivity, supporting the hypothesis that surface scattering dominates the return from the highlands. The maximum values of these polarization ratios are consistent with a significant component of multiple-bounce scattering. We calibrated the Arecibo backscatter values using areas of overlap with Magellan coverage, and found that the echo at high incidence angles (up to 70") from the highlands is lower than expected for a predominantly diffuse scattering regime. This behavior may be due to geometric effects in multiple scattering from surface rocks, but fur- ther modeling is required. Areas of lower radar backscatter above an upper critical elevation are found to be generally consistent across the equatorial highlands, with the shift in micro- wave properties occurring over as little as 5ÜÜ m of elevation. -
Cryovolcanism: Ice As Lava
Cryovolcanism: Ice as Lava Fernanda Scuderi University at Buffalo, Department of Geology, Buffalo, NY Abstract. Cryovolcanism, a new branch of planetary volcanology, was recently discovered when Voyager 2 identified geyser-like plumes of nitrogen on Neptune’s moon, Triton. Defined as the eruption of water and other liquid or vapor-phase volatiles onto the frigid surfaces of the outer solar system satellites, this form of exotic volcanism is a likely explanation for some of the volcanic-like features seen on the moons of Jupiter, Saturn, Uranus, and Neptune. Europa, Jupiter’s smallest moon, appears to be bristling with signs of recent activity, and is suspected of having a liquid water ocean beneath a water ice crust, ideal conditions for cryovolcanic activity. In combination with its peculiar smooth and ridged plains, Europa has relatively few impact craters indicating that the surface is comparatively young, as little as 100 million years old. This suggests that resurfacing has occurred, or may be still occurring today in the far reaches of the solar system, in which case cryovolcanism may be the answer. 1. Introduction 2. Cryomagmas The eruption of “ice” onto the surfaces Two conditions must exist for of planetary bodies, in a manner not unlike cryovolcanism to take place on the icy satellites: silicate volcanism, seems a bit strange in the way liquids must be generated in the interior, and then of temperature and composition. However, the melt must migrate to the surface. For this, the cryovolcanism is compatible with the American right planetary factors are needed: the size of the Geophysical Institute definition of volcanism, moon should be large enough for sufficient which refers to the extrusion of molten rock gravitational energy to generate heat for the without reference to composition. -
Possibility of Life on Jupiter's Moon
3/25/2020 Jupiter Solar System Sites that might support life! Jupiter and its Satellites Juno, Io & Europa Dr. Alka Misra Department of Mathematics & Astronomy University of Lucknow, Lucknow • • As massive as Jupiter is, though, it is Named after the most powerful god of still some 1000 times less massive the Roman pantheon, Jupiter is by far than the Sun. the largest planet in the solar system. • This makes studies of Jupiter all the • Ancient astronomers could not have more important, for here we have an known the planet's true size, but their object intermediate in size between the Sun and the terrestrial planets. choice of names was very appropriate. • It is 1.9×1027kg, or 318 Earth masses. • Jupiter is the third-brightest object in the night sky (after the Moon and Venus), making it very easy to locate • Jupiter has more than twice the and study mass of all the other planets combined. • Studies of the planet's internal • Knowing Jupiter's distance and structure indicate that Jupiter must angular size, we can easily be composed primarily of hydrogen determine its radius. and helium. • It is 71,400 km, or 11.2 Earth • Doppler-shifted spectral lines prove radii. that the equatorial zones rotate a little faster (9h50m period) than the • From the size and mass, we derive higher latitudes (9h56m period). an average density of 1300 kg/m3 (1.3 g/cm3) for the planet. • Thus, Jupiter exhibits differential rotation 1 3/25/2020 • Jupiter has the fastest rotation rate Atmosphere of the Jupiter of any planet in the solar system, and this rapid spin has altered • Jupiter is visually dominated by two features.